 |
|
|
|
|
|
|
|
|
|
|
|
|
| • |
The
NSF will only fund FASR if the US solar community tells them to.
|
|
|
In
order to achieve FASR, we have to persuade, primarily, the US solar
|
|
|
|
community
that it is a project that
will be useful to them
|
|
|
| • |
For
this reason we will make it as easy as possible for everyone to use
|
|
|
|
FASR
data: this means providing
images on demand
|
|
|
| • |
Original
version of FASR started at 500 MHz
for several reasons:
|
|
|
|
- we thought that 500 – 20000 MHz might
be technically feasible
|
|
|
|
with a single set of telescopes with a reasonable budget
|
|
|
|
- we had two strong science goals (flares
and coronal magnetic
|
|
|
|
fields) that could be addressed with this range
|
|
|
|
- little interest in lower frequencies in
the US: lack of relevance
|
|
|
|
to main science themes in US solar science
|
|
|
| • |
Frequency
ranges: 2 – 20 GHz: coronal
magnetic fields
|
|
|
|
2 – 30 GHz: flare gyrosynchrotron
emission
|
|
|
|
0.5 – 1 GHz: decimeter emission (no
imaging)
|
|
|
|
|
|